In Figure REF , we show the excess surface density
profiles derived from the g-g lensing signal for sample cAGN
and corresponding control samples cSF\(^{\rm c}\)  and cQ\(^{\rm c}\) . As one can see, the ESD
profiles obtained from cAGN and cSF\(^{\rm c}\)  are quite similar, while
that for cQ\(^{\rm c}\)  is higher. To quantify the results,
We use model M1 (see Section REF  and also [1]})
to fit the observed ESD profiles and to derive an average halo mass for each of the three
samples. The results of the halo mass are listed in Table REF .
The halo mass for central AGNs is about \(10^{11.85}\, h^{-1}{\rm M_\odot }\) ,
in agreement with the g-g lensing results for AGNs selected from the SDSS DR4
[2]}. The halo mass for the control sample of
star-forming galaxies, cSF\(^{\rm c}\) , is very similar to that of AGNs, while the mean
halo mass for the quiescent galaxies, about \(10^{12.38}\, h^{-1}{\rm M_\odot }\) , is about
three times as high as those for AGNs and star-forming galaxies
of the same stellar mass. We have also carried out the same analysis
for AGN hosts and normal galaxies in four stellar mass bins, and corresponding results
are listed in Table REF  and plotted in Figure.REF .
As expected, for each population, the average halo mass is larger for galaxies
with larger stellar masses. For a given stellar mass, the average halo
masses for AGN hosts and star-forming galaxies are similar but lower than
that of quiescent galaxies.
